Our work can be extended in various directions. The first obvious direction is considering more numerous and precise mass-radius data. There is an organized effort to extend the dataset we considered by using X-ray observations of more neutron stars [1]}, [2]}, [3]}. Similarly, future gravitational wave observations will also enrich the neutron star mass-radius measurements [4]}. Mass or radius measurements performed separately can also be useful, since they can be used to rule out certain ranges of parameters or EOS, for example by comparing the maximum allowed mass in a theory to the most massive neutron stars that have been observed [5]}. Incorporating such data into our analysis can increase the precision of our results, and potentially enable us to effectively constrain spontaneous scalarization in the \(m_{\phi }\ne 0\)  case as well.
